Table 3
Results of the fits of our simulated 511 keV emission spatial distributions to about 8 years of INTEGRAL/SPI observations.
| Model | Inner | Outer | All-Sky | MLR |
| component | component | component | ||
|
|
||||
| 26Al | 45.3±1.0 (0.85) | 1987 | ||
| 56Ni | 43.1±0.9 (1.93) | 2362 | ||
| All (=26Al+44Ti+56Ni) | 44.8±1.0 (1.39) | 2289 | ||
|
|
||||
| OB+26Al | 7.1±0.3 | 18.3±1.4 (3.57) | 2758 | |
| OB+56Ni | 6.2±0.3 | 18.5±1.5 (0.82) | 2731 | |
| OB+All | 6.4±0.3 | 19.0±1.6 (0.59) | 2743 | |
|
|
||||
| CMZ 26Al+OB+(SFD 26Al+56Ni) | 0.8±0.1 (3.35) | 5.8±0.3 | 17.0±1.6 (0.62) | 2759.8 |
|
|
||||
| UW (=IB+OB+Robin disk) | 1.44 ± 0.17 | 5.7 ± 0.3 | 13.9±1.3 | 2766.6 |
Notes. Column 1 gives the model or the combination of models fitted to the data. The SN Ia escape fraction for 56Ni positrons is 5%, and the halo GMF is the dipole field. Columns 2−4 give the fitted fluxes in 10-4 ph cm-2 s-1 for the inner bulge, outer bulge, and all-sky components. The numbers in parentheses are the scaling factors applied to our models in the fit. Column 5 gives the maximum likelihood ratio.
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